The interstellar environment of our galaxy

By K. Ferrière. 2001

725 citations recorded by the source corpus.

This article reviews the current knowledge and understanding of the interstellar medium of our galaxy. The author first presents each of the three basic constituents\char22{}ordinary matter, cosmic rays, and magnetic fields\char22{}of the interstellar medium, with emphasis on their physical and chemical properties as inferred from a broad range of observations. The interaction of these interstellar constituents, both with each other and with stars, is then discussed in the framework of the general galactic ecosystem.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/cae5307302493bf6fcdd83cd439fb4efeca6eafe

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Citations in the corpus

A High Spatial Resolution X-Ray and Hα Study of Hot Gas in the Halos of Star-forming Disk Galaxies. II. Quantifying Supernova Feedback (2003, background): “The mean number density and thermal pressure in normal star-forming spiral galaxies like the Milky Way or NGC 891 are n0 1 cm 3 and P=k 104 K cm 3, respectively (Ferrière 2001; Wolfire et al. 2003).”
Physical Processes in the Interstellar Medium (2014, methodology): “The information on the typical density and temperature ranges was taken from the review by Ferriére (2001), while the information on the typical fractional ionization of the various phases is based on Caselli et al. (1998), Wolfire et al. (2003), and Jenkins (2013).”
MOMENTUM INJECTION BY SUPERNOVAE IN THE INTERSTELLAR MEDIUM (2014, background): “Although observational estimates are difficult, the hot ISM is believed to fill a fraction 30% of the Milky Way disk’s volume (e.g., Ferriere 1998; Ferrière 2001; Könyves et al. 2007), with the majority filled by WNM (and embedded cold clouds).”
Are the Models for Type Ia Supernova Progenitors Consistent with the Properties of Supernova Remnants? (2007, methodology): “For the ISM parameters ISM and TISM we have chosen reference values typical of the warm atomic phase of the ISM: ISM ¼ 10 24 g cm 3 and TISM ¼ 104 K (Ferrière 2001).”
MAXIMALLY STAR-FORMING GALACTIC DISKS. I. STARBURST REGULATION VIA FEEDBACK-DRIVEN TURBULENCE (2011, result): “…of highly-supersonic magnetohydrodynamic turbulence (e.g. Stone et al. 1998; Mac Low et al. 1998) have shown that the magnetic energy is typically smaller than the turbulent energy by a factor ∼ 2 − 3, so that B2midplane/(8π) <∼ ρ0〈v2z〉; this is also consistent with observations (Ferrière 2001).”
THE THREE-PHASE INTERSTELLAR MEDIUM REVISITED (2005, methodology): “…as noted, all estimates in this article of the distributions of interstellar densities, supernova rates, etc., with distance from the midplane, z, are those adopted in the excellent review by Ferrière (2001); no further reference is made here to the invaluable original sources of this information.”
Energy spectra of the soft X-ray diffuse emission in fourteen fields observed with Suzaku (2009, background): “The Ovii emission of the M12on field must arise from the near side of the MBM-12 molecular cloud whose distance is 60 - 300 pc. Assuming the midplane space-averaged neutral density (Ferrière 2001), the absorption length of Ovii emission is estimated to be 300 pc for MP235.”
VERTICAL STRUCTURE OF A SUPERNOVA-DRIVEN TURBULENT, MAGNETIZED INTERSTELLAR MEDIUM (2012, methodology): “If we assume that ∼30% of the warm gas in our simulation is ionized (Ferrière 2001) while the cool gas is all neutral, thermally unstable gas accounts for ∼40% of the mass in the range 200 K T 104.2 K in our magnetized and unmagnetized simulations.”
THE PHYSICS OF THE FAR-INFRARED–RADIO CORRELATION. I. CALORIMETRY, CONSPIRACY, AND IMPLICATIONS (2009, methodology): “…disk with R = 4 kpc, and a surface density of Σg = 0.01 g cm −2 derived from the Schmidt law (Section 2.2) and the Milky Way luminosity, L⋆ ≈ 2 × 1010L⊙ (Freudenreich 1998; similar results are obtained by using the starlight radiation field in Strong et al. 2000, or the SN rate in Ferrière 2001).”
Cosmic ray transport in the Galaxy: A review (2017, background): “For typical ISM conditions (T4 = 1, B0 = 3µG, ni = 0.45 cm −3 and nH = 0.05 cm −3 (Ferrière, 2001)) the critical wavenumber turns out to be kc = 4.5 × 10−15cm−1, corresponding, through the resonance condition to a particle rigidity Rc ≈ 200 GV.”
Modelling CO emission – I. CO as a column density tracer and the X factor in molecular clouds (2010, background): “…environment corresponding to the simulated cloud: a high density cloud found in the galactic center (n1000), a typical Milky Way cloud (n300, Ferrière 2001), clouds in low metallicity systems like the LMC or SMC (n300-Z03 and n300-Z01), a low density cloud in a dwarf galaxy (n100), and…”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, methodology): “The ISM is a spatially inhomogeneousenvironment consisting of several phases that have different temperatures, denities and degrees of ionization (Ferrière 2001).43 We will use the Warm ISM phase (see Table 1) as our fiducial interstellar plasma and discuss briefly what is known about the two main…”
Cosmic-ray propagation with DRAGON2: I. numerical solver and astrophysical ingredients (2016, methodology): “For the source term we choose the Ferriere2001 model, with a slope for momentum of 2.3.”
The 511 keV emission from positron annihilation in the Galaxy (2010, methodology): “III (e.g. Ferriere, 44 1998; Ferrière, 1999, 2001; McKee and Ostriker, 1977) is needed.”
Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks (2009, background): “We follow Ferrière (2001) and consider molecular gas (as traced, e.g., via its CO emission), as well as atomic hydrogen gas (as observed, e.g., by its 21 cm emission).”
Simulations of the Small-Scale Turbulent Dynamo (2003, neutral): “…& Spangler 1996; Zweibel & Heiles 1997; Vallée 1997, 1998; Balbus & Hawley 1998; Kulsrud 1999; Weiss & Tobias 2000; Title 2000; Beck 2000, 2001; Ferrière 2001; Kronberg et al. 2001; Carilli & Taylor 2002; Han & Wielebinski 2002; Widrow 2002; Tobias 2002; Ossendrijver 2003; Han et al. 2004;…”